ALMA CARMA

Interferometric Arrays During Spitzer and Beyond

EVLASMA

Lee Mundy, University of Maryland

EVLA – An Upgrade to the VLA

– frequency: 1 - 50 GHz– sensitivity: 1 µJy in 12 hours– resolution: 10 masec @ 20

GHz (Phase II)– brightness sensitivity: 0.1 mK

@ 10 GHz @ 10"– new correlator:

• 16384 channels at full bandwidth,

• 4.2M channels at highest spectral resolution;

More sensitive, higher resolution, better frequency coverage, better correlator

EVLA Sensitivity

Current VLACurrent VLA

EVLA EVLA

Factors of 20 to 50 better at high frequencies in the continuum

Phased Deployment

Phase I - hardware, electronics, correlator, and softwarecurrently funded at $5M/year for completion in 2012

Phase II - 8 new antennas, 20 new close-packed padsproposal just went in to NSF. Could also be completed by 2012 if funded soon.

Why improve the VLA ?

•Non-thermal processes emit at cm-wavelengths

•Lower dust opacity at long λ

•Cosmic expansion shifts spectrum to longer λ

At z > 1.5 the low J CO lines shift into the EVLA bands

Why both EVLA and ALMA?

• The inner disks are optically thick at mm λ

• cm and mm emission can trace difference physical processes: winds, shocks and ionized gas versus dust

• Coordinated attack on inner disk and wind

OVRO

BIMA

Berkeley – Illinois – MarylandNine 6.1 m dishes

ChicagoEight 3.5 m dishes

Combined Array for Research in Millimeter Astronomy

Caltech Six 10.4 m dishes

New CARMA SiteInyo National ForestCedar Flat – 7300’

CARMA D Array + SZA

CARMA Sensitivity

4 K67 K0.2”4.5 K77 K0.4”A

1.0 K17 K0.4”0.7 K12 K1.0”B

0.13 K2.2 K1.1”0.1 K2.0 K2.5”C

0.02 K0.4 K2.7”0.02 K0.3 K6.3”D

5-hr1-minBeam5-hr1-minBeamArray

GHz230GHz100 Line:1 km/sec

0.07 mJy1.1 mJy0.04 mJy0.7 mJy

5-hr1-min5-hr1-min

GHz230GHz100

Continuum

Factor of 5 to 20 better than BIMA/OVRO Arrays

High resolutionHigh sensitivity

2 km baselines – 0.12” @1mm

CO

R

Hα

NGC 4826 NGC 5055 NGC 5194 NGC 7331

Unbarred galaxies in BIMA SONG Survey

Central kpc

Large bandwidth, high sensitivity

Timeline

2003 December2004 June2004 Summer 2004 Fall2005 Fall

• Cedar Flat permit• Shut down BIMA & OVRO• Roads, pads, buildings• Move BIMA & OVRO• First light & Operations

The SubMillimeter Array on Mauna Kea

SAO andASIAA

SMA Receiver Bands

230230GHzGHz

345345GHzGHz

690690GHzGHz

460460GHzGHz

820820GHzGHz

NextNextbandband

Solar System: Titan

M. M. GurwellGurwellTitan Atmosphere is Rich in Different Molecular Species

Titan

Young Star: L1551 Gas ImageGas ImageSubmm Line Picks up Warm Dense Core Within Cooler Envelope

(> 60 K) (> 107cm-3) (700 AU)

CS 7CS 7--66

S. S. TakakuwaTakakuwa

CircumbinaryCircumbinary Disk ?Disk ?

Gas Shows Rotational Motions

C18O (1-0) CS (7-6)

Motion Dominated by Motion Dominated by KeplerKepler Rotation at 100 AU ScaleRotation at 100 AU Scale

Interacting System VV114CO J=2-1 very similar to J=1-0; CO J=3-2 picks out Hot Core

CO(3-2) CO(2-1)

CO(1-0) M1/M2

D = 77 Mpc

LIR = 4.0 x 1011 Lsun

MH2 = 5.1 x 1010 Msun

Late stage merger

D. D. IonoIono

ALMA Atacama Large Millimeter Array

ALMA

ALMA is an equal partnership between Europe and North America, in cooperation with the Republic of Chile, and is funded by:- the U.S. National Science Foundation (NSF), - the National Research Council of Canada (NRC), - the European Southern Observatory (ESO), and Spain.

ALMA construction and operations are led on behalf of Europe by ESO, and on behalf of North America by the National Radio Astronomy Observatory (NRAO), which is managed by Associated Universities, Inc. (AUI).

ALMA Scope

Antennae 64 × 12 mcollecting area > 7000 m2

Configurations 150 m – 14 kmresolution (300 GHz) 1.4 – 0.015"

Frequency 31 – 950 GHzwavelength 10 – 0.3 mm

Receiver sensitivity close to quantum limitCorrelator 16 GHz / 4096 chan.Site excellentTotal Cost (FY2000 $) 562M USD

A leap of over two orders of magnitude in both spatial resolution and sensitivity

Site in Northern Chile

High Atacama Desert:low water vapor, moderate climate,good access

ALMA Site:Chajnantor

ALMA FE key specifications

SIS

SIS

SIS

SIS

SIS

SIS

SIS

SIS

HEMT

HEMT

Receiver technology

787 – 950 GHz

602 – 720 GHz

385 – 500 GHz

275 – 370 GHz

211 – 275 GHz

163 - 211 GHz

125 – 163 GHz

84 – 116 GHz

67 – 90 GHz

31.3 – 45 GHz

Frequency Range

328 K219 K655 K438 K10

250 K168 K500 K335 K9

135 K91 K270 K181 K8

99 K67 K198 K133 K7

63 K39 K126 K77 K6

49 K30 K98 K60 K5

38 K24 K76 K47 K4

27 K17 K54 K34 K3

22 K14 K43 K28 K2

12 K8 K23 K15 K1

TDSB at any RF frequency

TDSB over 80% of the RF band

TSSB at any RF frequency

TSSB over 80% of the RF band

Receiver noise temperature / DSBReceiver noise temperature / SSBALMABand

•Dual, linear polarization channels:•Increased sensitivity•Measurement of 4 Stokes parameters

•183 GHz water vapour radiometer:•Used for atmospheric path length correction

ALMA Prototype Antennas in Testing

ALCATEL/EIE Prototype VertexRSI Prototype

The Chajnantor plateau

Construction has begun

The Chajnantor plateau in the future

AOS Configurations

AOS Configurations

ALMA Median Sensitivity in 60 seconds

230

12.61.1.06753.316.0.23452.110.0.101.47.00.05110

Line 25 km s-1

(mJy)Line 1 km s-1

(mJy)Continuum

(mJy)Frequency

(GHz)

Point source sensitivity

0.030.170.0036750.030.180.0023450.50.240.0022300.140.700.005110

Line 25 km s-1

(K)Line 1 km s-1

(K)Continuum

(K)Frequency

(GHz)

Brightness Temperature1” beam

Planetary Atmospheres and Surfaces - Io’s Volcanism

Io: 3630 km diameter= 1” at 5 AU

500 km plume = 140 mas Galileo images courtesy NASA/JPL-Caltech

ALMA can map thermal emission from the surface showing location and temperature of hot spots, and can map

molecules in volcanic plumes

Planetary Surfaces -Mapping Pluto and Charon

Pluto is 100 mas and Charon is 50 mas at current distance from

sun.

ALMA will map the thermal emission from Pluto and Charonwith up to 40 resolution elements, measuring temperature

and/or emissivity variations that may change with time

Circumstellar Disks and Early Planet Formation

L. G. Mundy

Simulation Contains:* 140 AU, 0.01 solar mass disk* inner hole (3 AU)* gap 6-8 AU* forming giant planets at:

9, 22, 46 AU with localover-densities

* ALMA with 2x over-density* ALMA with 20% under-density* Each letter 4 AU wide, 35 AU highObserved with 10 km array at 140 pc, 1.3 mmALMA can detect an 0.001 solar mass circumstellar disk in Orion in 60 seconds in dust emission.

ALMA can map disks at 0.1” resolution with 0.01K continuum and 1 K line sensitivity at 345 GHzObserved Model

Planets and Debris Disks

SMM image of Vega (JCMT by Holland et al.)at 850 microns with 15” resolution

Model by (Wyatt 2003) as star, Neptune-like planet, and debris disk

Vega at 1300 microns with 5” resolution (Wilner et al. 2003). Model of resonance with planet.

ALMA can detect the Vega disk in a few seconds and will have thesensitivity to map the emission at better than 0.5” resolution.

Detecting Dust Emission from Galaxies as all Z’s

ALMA will detect large numbers of galaxies at all Z, beating the confusion limit

ALMA will probe dust and molecular gas emission during the period of most active galaxy formation, z=2-4

Submm galaxies in CO(3-2),(4-3)

ALMA’s spatially and spectrally resolved images will reveal the massesand dynamics during galaxy assembly

Frayer et al. N4 Smail et al. N2.4Chapman et al.

Fine angular scale CMB and SZ

X-ray

SZ effect

ALMA compact array will be extremely sensitive to arcmin-scale CMB power from clusters, filaments and primordial fluctuations

ALMA Carlstrom et al. witharcmin resolution Chandra – low-z Hydra

cluster with substructure

Fine resolution will reveal structure in the intracluster medium to resolve physical

conditions in cluster gas

ALMA Schedule

1998 – 2002 Design and Development2003 Bilateral Agreement between NSF and ESO

signed2003Completion of Proto-type Antennas2004 Ground Breaking2004 Site construction, antenna contract awarded2004 Japan joins 2005 First production antenna in Chile2007 Q3 Early science operation begins, 8 antennas2011 End construction2012 Full science operations

ALMA 2012